Spectral and Timing Evolution of the Black Hole X-Ray Nova 4U 1543–47 during Its 2002 Outburst
Spectral and Timing Evolution of the Black Hole X-Ray Nova 4U 1543–47 during Its 2002 Outburst
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DOI：
10.1086/421511
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发表时间：
2003-08
期刊：
影响因子：
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通讯作者：
S. Park;Jon M. Miller;J. E. McClintock;Ron Remillard;J. Orosz;C. Shrader;R. Hunstead;D. Campbell-Wilson;C. Ishwara-Chandra;A. Rao;M. Rupen
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文献类型：
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作者：
S. Park;Jon M. Miller;J. E. McClintock;Ron Remillard;J. Orosz;C. Shrader;R. Hunstead;D. Campbell-Wilson;C. Ishwara-Chandra;A. Rao;M. Rupen
我们提出了一个X射线光谱和定时分析4U 1543-47在其2002年爆发的基础上获得的49点观测使用罗西X射线定时探测器。爆发在2-12千电子伏波段达到了4.2克拉布的峰值强度，并在整个为期一个月的观测中下降了32倍。在X射线极大值前两天，在1026.75 MHz探测到一个21.9 ± 0.6 mJy的射电耀斑;在爆发后期，X射线源进入“硬”状态后，也探测到了射电源。X射线光变曲线呈现出快速上升和指数衰减的经典形状。光谱是软的，主要是吸积盘的辐射。该连续谱符合一个圆盘黑体（kTmax = 1.04 keV）和幂律（Γ ~ 2.7）。在衰变阶段的中途，一个强烈的低频准周期振荡（ν = 7.3-8.1 Hz）持续了几天。该光谱具有不对称的宽Fe Kα线，表明该线是由于相对论增宽而不是康普顿化引起的。相对论性的Laor模型比非相对论性的Gaussian模型更好地拟合这条线，特别是在我们观察的开始和结束附近。线拟合得到的内盘半径估计值在6 Rg以内;这个结果和其他证据表明这个黑洞可能有非零的角动量。
We present an X-ray spectral and timing analysis of 4U 1543-47 during its 2002 outburst based on 49 pointed observations obtained using the Rossi X-Ray Timing Explorer. The outburst reached a peak intensity of 4.2 crab in the 2-12 keV band and declined by a factor of 32 throughout the month-long observation. A 21.9 ± 0.6 mJy radio flare was detected at 1026.75 MHz two days before the X-ray maximum; the radio source was also detected late in the outburst, after the X-ray source entered the "hard" state. The X-ray light curve exhibits the classic shape of a rapid rise and an exponential decay. The spectrum is soft and dominated by emission from the accretion disk. The continuum is fitted with a multicolor disk blackbody (kTmax = 1.04 keV) and a power law (Γ ~ 2.7). Midway through the decay phase, a strong low-frequency quasi-periodic oscillation (ν = 7.3-8.1 Hz) was present for several days. The spectra feature a broad Fe Kα line that is asymmetric, suggesting that the line is due to relativistic broadening rather than Comptonization. Relativistic Laor models provide much better fits to the line than nonrelativistic Gaussian models, particularly near the beginning and end of our observations. The line fits yield estimates for the inner disk radius that are within 6Rg; this result and additional evidence indicates that this black hole may have a nonzero angular momentum.